Magnetic field generation in fully convective rotating spheres

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dc.creatorDobler, W.
dc.creatorStix, M.
dc.creatorBrandenburg, A.
dc.date2004-10-27
dc.date2006-01-19
dc.date.accessioned2026-07-07T06:37:05Z
dc.date.available2026-07-07T06:37:05Z
dc.descriptionMagnetohydrodynamic simulations of fully convective, rotating spheres with volume heating near the center and cooling at the surface are presented. The dynamo-generated magnetic field saturates at equipartition field strength near the surface. In the interior, the field is dominated by small-scale structures, but outside the sphere by the global scale. Azimuthal averages of the field reveal a large-scale field of smaller amplitude also inside the star. The internal angular velocity shows some tendency to be constant along cylinders and is ``anti-solar'' (fastest at the poles and slowest at the equator).
dc.description12 pages, 11 figures, 2 tables, to appear in the 10 Feb issue of ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0410645
dc.identifierhttp://arxiv.org/abs/astro-ph/0410645
dc.identifierAstrophys.J. 638 (2006) 336-347
dc.identifierdoi:10.1086/498634
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/100271
dc.subjectAstrophysics
dc.titleMagnetic field generation in fully convective rotating spheres
dc.typetext

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